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2MASS J15104761–2818234, sometimes shortened to 2M1510, is a triple or possibly quadruple brown dwarf system, consisting of the eclipsing binary 2M1510A and the wide companion 2M1510B.[1] 2M1510A was found to be an eclipsing binary in the first light data of the SPECULOOS telescopes. It is only the second eclipsing binary brown dwarf found so far (as of March 2020), the other is 2M0535-05. The system verified theoretical models for how brown dwarfs cool. The system is located 120 light-years away from earth in the constellation Libra.[5]
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Libra |
| 2M1510 A | |
| Right ascension | 15h 10m 47.86s[2] |
| Declination | −28° 18′ 17.5″[2] |
| Apparent magnitude (V) | |
| 2M1510 B | |
| Right ascension | 15h 10m 47.60s[3] |
| Declination | −28° 18′ 23.4″[3] |
| Apparent magnitude (V) | |
| Characteristics | |
| 2M1510 A | |
| Spectral type | M9γ + L1β(?) (near-IR)[1][4] |
| Apparent magnitude (G) | 17.487[2] |
| Variable type | eclipsing[1] |
| 2M1510 B | |
| Spectral type | M9γ (near-IR)[1] |
| Apparent magnitude (G) | 18.886[3] |
| Astrometry | |
| 2M1510 A | |
| Radial velocity (Rv) | -12.9 ± 0.4[1] km/s |
| Proper motion (μ) | RA: −118.747±0.492[2] mas/yr Dec.: −46.865±0.420[2] mas/yr |
| Parallax (π) | 27.2203 ± 0.2665 mas[2] |
| Distance | 120 ± 1 ly (36.7 ± 0.4 pc) |
| 2M1510 B | |
| Radial velocity (Rv) | -12.0 ± 0.3[1] km/s |
| Proper motion (μ) | RA: −117.458±0.893[3] mas/yr Dec.: −45.713±0.746[3] mas/yr |
| Parallax (π) | 27.6869 ± 0.4939 mas[3] |
| Distance | 118 ± 2 ly (36.1 ± 0.6 pc) |
| Orbit[1] | |
| Primary | 2M1510 Aa |
| Companion | 2M1510 Ab |
| Period (P) | 20.9022+0.0059 −0.0056 days |
| Semi-major axis (a) | 0.0627 ± 0.0014 au |
| Eccentricity (e) | 0.309 ± 0.022 |
| Inclination (i) | 88.5 ± 0.1° |
| Details[1] | |
| 2M1510 Aa | |
| Mass | 0.0382+0.0028 −0.0026 M☉ |
| Radius | 1.575 RJup |
| Luminosity | 0.00063±0.00001 L☉ |
| Surface gravity (log g) | 4.55 cgs |
| Temperature | 2,400 K |
| Rotational velocity (v sin i) | 8.7±1.0 km/s |
| Age | 45 ± 5 Myr |
| 2M1510 Ab | |
| Mass | 0.0375+0.0029 −0.0028 M☉ |
| Radius | 1.575 RJup |
| Luminosity | 0.00063±0.00001 L☉ |
| Surface gravity (log g) | 4.55 cgs |
| Temperature | 2,400 K |
| Metallicity [Fe/H] | 0.0 dex |
| Rotational velocity (v sin i) | 6.8±1.5 km/s |
| Age | 45±5 Myr |
| Other designations | |
2M1510 AB, 2MASSW J1510478–281817, 2MASS J15104761–2818234, DENIS J151047.8–281817, 2MUCD 20604, Gaia DR2 6212595980928732032 | |
| Database references | |
| SIMBAD | A |
| B | |
Signs of youth
2M1510A has hydrogen-alpha emission lines, which is interpreted as a sign of youth.[6] The system also belongs to the 45±5 million-year-old Argus moving group[7] and the brown dwarfs have a low surface gravity, which is an additional indicator for youth.[1]
The brown dwarf system
2M1510A and 2M1510B are separated by 250 astronomical units, making them a resolved binary in 2MASS data. The components of the inner eclipsing binary are called 2M1510Aa and 2M1510Ab. Despite the small letter used in this configuration these objects are not planets, but brown dwarfs that burn deuterium. 2M1510A is not only an eclipsing binary, but also a double-lined spectroscopic binary. This was discovered by follow-up observations with Keck II. Follow-up observations with Keck II and the VLT UT2 showed that 2M1510Aa and 2M1510Ab have very similar masses, something that is called a near equal-mass binary. 2M1510Aa has a mass of about 40 MJ and 2M1510Ab has a mass of about 39 MJ. The pair orbits each other every 20.9 days.[1] Additionally the 2M1510A source has an elongated PSF in VLT/SINFONI data. The naming of the brown dwarfs in Calissendorff et al. 2019 does not follow other works and the companion was called 2M1510B (here from now on: 2M1510B'). 2M1510B' has a mass of 17.68+4.20
−2.10 MJ and it is separated by about 4.4 au from 2M1510A and orbits the eclipsing binary each 30 years.[4] This result was not considered by Triaud et al. 2020 and it could represent a contamination of the eclipsing binary, making a test of the cooling models more challenging.
See also
- List of nearby stellar associations and moving groups
- W2150AB another wide binary
- DENIS-P J020529.0−115925 another triple brown dwarf system
References
- Triaud, Amaury H. M. J.; Burgasser, Adam J.; Burdanov, Artem; Kunovac Hodžić, Vedad; Alonso, Roi; Bardalez Gagliuffi, Daniella; Delrez, Laetitia; Demory, Brice-Olivier; de Wit, Julien; Ducrot, Elsa; Hessman, Frederic V. (January 2020). "An Eclipsing Substellar Binary in a Young Triple System discovered by SPECULOOS". Nature Astronomy. 4 (7): 650–657. arXiv:2001.07175. Bibcode:2020NatAs.tmp...43T. doi:10.1038/s41550-020-1018-2. S2CID 210839528.
- Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- Calissendorff, Per; Janson, Markus; Asensio-Torres, Rubén; Köhler, Rainer (July 2019). "Spectral characterization of newly detected young substellar binaries with SINFONI". Astronomy & Astrophysics. 627: A167. arXiv:1906.05871. Bibcode:2019A&A...627A.167C. doi:10.1051/0004-6361/201935319. ISSN 0004-6361. S2CID 189898015.
- "Astronomers Catch Rare Eclipse of a Double Brown Dwarf System – W. M. Keck Observatory". Retrieved 2020-03-10.
- Gizis, John E. (August 2002). "Brown Dwarfs and the TW Hydrae Association". The Astrophysical Journal. 575 (1): 484–492. arXiv:astro-ph/0204342. Bibcode:2002ApJ...575..484G. doi:10.1086/341259. ISSN 0004-637X. S2CID 119091936.
- Gagné, Jonathan; Faherty, Jacqueline K.; Cruz, Kelle L.; Lafreniére, David; Doyon, René; Malo, Lison; Burgasser, Adam J.; Naud, Marie-Eve; Artigau, Étienne; Bouchard, Sandie; Gizis, John E. (August 2015). "BANYAN. VII. A New Population of Young Substellar Candidate Members of Nearby Moving Groups from the BASS Survey". The Astrophysical Journal Supplement Series. 219 (2): 33. arXiv:1506.07712. Bibcode:2015ApJS..219...33G. doi:10.1088/0067-0049/219/2/33. ISSN 0067-0049. S2CID 117788987.
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На других языках
- [en] 2M1510
[ru] 2M1510
2M1510 — тройная или, возможно, четверная система из коричневых карликов, состоит из затменно-двойной звезды 2M1510A и удалённого компаньона 2M1510B[5]. 2M1510A оказалась затменной двойной звездой, сведения об этом были получены при обработке первых данных телескопов SPECULOOS. По состоянию на начало марта 2020 года это только вторая известная затменная двойная звезда, состоящая из коричневых карликов, второй является 2M0535-05. Данные об объекте подтвердили теоретические модели охлаждения коричневых карликов. Звёздная система расположена на расстоянии 120 световых лет от Солнца в созвездии Весов[9].Другой контент может иметь иную лицензию. Перед использованием материалов сайта WikiSort.org внимательно изучите правила лицензирования конкретных элементов наполнения сайта.
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